Neutrino Astronomy. Ph 135 Scott Wilbur

Transcription

1 Neutrino Astronomy Ph 135 Scott Wilbur

2 Why do Astronomy with Neutrinos? Stars, active galactic nuclei, etc. are opaque to photons High energy photons are absorbed by the CMB beyond ~100 Mpc ev protons, which should be created with neutrinos, have been seen Can be used to observe possible dark matter reactions In short: we can probe new phenomena and look farther back

3 Why do Astronomy with Neutrinos? Three main areas of research: Astronomy More information about high-energy protons and γ rays Particle Physics Extremely long baseline for neutrino oscillation studies Dark Matter Searches Many dark matter candidates would leave neutrino signatures

4 The Detector A neutrino interacts with matter in the telescope, creating a muon or a hadronic or electromagnetic shower The muon (or shower) emits Cherenkov radiation as it travels through the ice Photomultipliers pick up the Cherenkov radiation and can infer the direction of travel To select only neutrino events, only tracks coming through the Earth are kept

5 The Detector Picture from AMANDA II Web Site:

6 Advantages of Neutrino Astronomy Can see through nearly anything Wide viewing angle

7 Disadvantages of Neutrino Astronomy Need gigantic telescopes Still see very few events

8 AMANDA Many arrays (A, B10, and II) at the South Pole Operational since January 1997

9 ANTARES Astronomy with a Neutrino Telescope and Abyss environmental RESearch Currently under construction, 5/12 strings completed 1000 photomultipliers, 0.1 km 2 planned Data will combine with AMANDA to provide better sky coverage

10 IceCube Next generation of neutrino telescopes 4200 photomultipliers, 1 km 2 telescope area 1 O angular resolution for muons, 10 O for showers 30% resolution in log of energy for muons, 20% in energy for showers

11 Astronomy Extremely high energy protons (over ev) have been observed Expected to come from supernova remnants and neutron stars accreting matter from companions These processes are expected to generate neutrinos as well, which would point back to their source

12 Astronomy Active Galactic Nuclei are the most luminous ( W known objects in the Universe ( Some emit relativistic jets with γ rays exceeding ev Theoretical models of AGNs have large uncertainties Any observations of these sources (such as neutrino emissions) are helpful

13 Astronomy γ ray bursts are extremely violent releases of ( alone energy (10 45 J in ~1 sec in γ rays We don't have a good theory about the mechanism of γ ray bursts By observing the afterglow, we can determine what happens, but not how it starts

14 Neutrino Physics A neutrino telescope can see atmospheric neutrinos produced on the other side of the Earth This gives a very long baseline for neutrino oscillation observations Much more accurate neutrino oscillation measurements, possibly including a sterile neutrino

15 Dark Matter Searches WIMPs can get trapped in gravity wells and annihilate at great rates γ rays would be absorbed, but neutrinos could be detected Neutrinos have energies 1/3-1/2 of WIMP mass Kaluza-Klein dark matter annihilates into neutrinos at a higher rate than WIMPs

16 Dark Matter Searches Both dark matter candidates would lead to an increased neutrino rate from the Sun: r qr 1= 0.3 r qr 1= 0.2 r qr 1= 0.1

17 Possible Exotic Results Neutrino telescopes are essentially detectors for extremely high energy accelerators (10 ( PeV We might see new physics at energy scales this high

18 Quantum Gravity Earth becomes opaque above ~100 TeV Angular distribution can give cross section Don't need known luminosity of source

19 Magnetic Monopoles Magnetic monopoles would have a large equivalent charge Cherenkov radiation goes as charge squared AMANDA has improved the bound on monopole flux density

20 References Francis Halzen, Astroparticle Physics with High Energy Neutrinos: from AMANDA to IceCube Dan Hooper, High Energy Neutrino Astronomy: Opportunities for Particle Physics Gianfranco Bertone, Dan Hooper and Joseph Silk, Particle Dark Matter: Evidence, Candidates and Constraints ANTARES web site: